Radiatively Inefficient Accretion Flow Models of Sgr A*

Details Radiatively Inefficient Accretion Flow Models of Sgr A* Radiatively Inefficient Accretion Flow Models of Sgr A*

2003-04-05

arxiv.org/abs/astro-ph/0304099v1

Astron.Nachr. 324S1 (2003) 435-443

Astronomy and Astrophysics

Astrophysics

9 pages; to appear in Astron. Nachr., Vol. 324, No. S1 (2003), Special Supplement "The central 300 parsecs of the Milky Way",

Scientific paper

10.1002/asna.200385043

I review radiatively inefficient accretion flow models for the 2.6 million solar mass black hole (BH) in the Galactic Center. I argue for a 'concordance model' of Sgr A*: both theory and observations suggest that hot ambient gas around the BH is accreted at a rate of order 10^{-8} solar masses/year, much less than the canonical Bondi rate. I interpret Chandra observations of Sgr A* in the context of such a model: (1) the extended 'quiescent' X-ray emission is due to thermal bremsstrahlung from gas in the vicinity of the Bondi accretion radius, and (2) the ~ ksec long X-ray flares are due to synchrotron or Inverse-Compton emission by non-thermal electrons accelerated in the inner 10 Schwarzschild radii of the accretion flow.

Affiliated with

Also associated with

No associations

Rating

Radiatively Inefficient Accretion Flow Models of Sgr A* does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Radiatively Inefficient Accretion Flow Models of Sgr A*, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radiatively Inefficient Accretion Flow Models of Sgr A* will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-143223